Quiescent and outburst photometry of the dwarf nova SS Cygni

Details Quiescent and outburst photometry of the dwarf nova SS Cygni Quiescent and outburst photometry of the dwarf nova SS Cygni

Feb 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989mnras.236..727h&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 236, Feb. 1, 1989, p. 727-734.

Astronomy and Astrophysics

Astronomy

17

Astronomical Photometry, Dwarf Novae, Light Curve, Stellar Models, Balmer Series, Cataclysmic Variables, Cygnus Constellation, Eclipsing Binary Stars

Scientific paper

Photometric observations of a wide and a narrow outburst of the dwarf nova SS Cygni are used to test the hypothesis that the same mechanism is responsible for the wide outbursts of U Gem stars and the wide outbursts of SU UMa stars. A search for modulations at or near the orbital period of the SS Cygni outbursts was conducted, showing no modulations to a limit of about 0.05 mag. The results are interpreted by Whitehurst's (1984) tidal superhump model which suggests that SU UMa and U Gem outbursts are manifestations of the same basic driving mechanism, but that the presence of superhumps is limited to extreme mass-ratio systems.

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